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Polar ionospheric responses to solar wind IMF changes

Polar ionospheric responses to solar wind IMF changes Auroral and airglow emissions over Eureka (89° CGM) during the 1997/98 winter show striking variations in relation to solar wind IMF changes. The period January 19 to 22, 1998, was chosen for detailed study, as the IMF was particularly strong and variable. During most of the period, B z was northward and polar arcs were observed. Several overpasses by DMSP satellites during the four day period provided a clear picture of the particle precipitation producing the polar arcs. The spectral character of these events indicated excitation by electrons of average energy 300 to 500 eV. Only occasionally were electrons of average energy up to ∼1 keV observed and these appeared transitory from the ground optical data. It is noted that polar arcs appear after sudden changes in IMF B y , suggesting IMF control over arc initiation. When B y is positive there is arc motion from dawn to dusk, while B y is negative the motion is consistently dusk to dawn. F-region (anti-sunward) convections were monitored through the period from 630.0 nm emissions. The convection speed was low (100/150 m/s) when B z was northward but increased to 500 m/s after B z turned southward on January 20. http://www.deepdyve.com/assets/images/DeepDyve-Logo-lg.png Annales Geophysicae Springer Journals

Polar ionospheric responses to solar wind IMF changes

Zhang, Y.; McEwen, D.; Guo, W.; Anderson, P.
Annales Geophysicae , Volume 18 (6) – Jan 1, 2000
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Publisher
Springer Journals
Copyright
Copyright © 2000 by EGS – Springer-Verlag
Subject
Earth Sciences; Geophysics/Geodesy; Astronomy, Observations and Techniques; Astrophysics and Astroparticles; Space Sciences (including Extraterrestrial Physics, Space Exploration and Astronautics)
ISSN
0992-7689
eISSN
1432-0576
DOI
10.1007/s00585-000-0629-2
Publisher site
See Article on Publisher Site

Abstract

Auroral and airglow emissions over Eureka (89° CGM) during the 1997/98 winter show striking variations in relation to solar wind IMF changes. The period January 19 to 22, 1998, was chosen for detailed study, as the IMF was particularly strong and variable. During most of the period, B z was northward and polar arcs were observed. Several overpasses by DMSP satellites during the four day period provided a clear picture of the particle precipitation producing the polar arcs. The spectral character of these events indicated excitation by electrons of average energy 300 to 500 eV. Only occasionally were electrons of average energy up to ∼1 keV observed and these appeared transitory from the ground optical data. It is noted that polar arcs appear after sudden changes in IMF B y , suggesting IMF control over arc initiation. When B y is positive there is arc motion from dawn to dusk, while B y is negative the motion is consistently dusk to dawn. F-region (anti-sunward) convections were monitored through the period from 630.0 nm emissions. The convection speed was low (100/150 m/s) when B z was northward but increased to 500 m/s after B z turned southward on January 20.

Journal

Annales Geophysicae – Springer Journals

Published: Jan 1, 2000

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